Evolution of massive stars and the origin of the elements

Journal Article · Tue Jan 01 00:00:00 EST 1980 · Energy Technol. Rev.; (United States)

OSTI ID:6769735

The first 8 to 14 million years in the life of a massive star are considered, in which its initial composition of hydrogen is hydrostatically burned into a sequence of heavier elements ending with iron. Models of 15 and 25 solar masses are examined with regard to pre-supernova evolution and structure, core collapse, and shock-wave formation. Explosive nucleosynthesis is also discussed, considering peak shock temperatures and zones of explosive neon burning. Attention is given to type II supernova light curves, supernova expansion velocities, energy losses from neutrino emission, degeneracy pressure, gravitational contraction, and iron photodisintegration.

• OSTI ID: 6769735
• Journal Information: Energy Technol. Rev.; (United States), Journal Name: Energy Technol. Rev.; (United States)
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
SUPERMASSIVE STARS
CHEMICAL COMPOSITION
STAR EVOLUTION
COSMIC NEUTRINOS
ENERGY LOSSES
GRAVITATIONAL COLLAPSE
NUCLEOSYNTHESIS
SHOCK WAVES
SUPERNOVAE
COSMIC RADIATION
ELEMENTARY PARTICLES
ERUPTIVE VARIABLE STARS
FERMIONS
IONIZING RADIATIONS
LEPTONS
LOSSES
MASSLESS PARTICLES
NEUTRINOS
RADIATIONS
STARS
VARIABLE STARS
640106* - Astrophysics & Cosmology- Cosmology